Perturbation theory approach to predict the covariance matrices of the galaxy power spectrum and bispectrum in redshift space
Perturbation theory approach to predict the covariance matrices of the galaxy power spectrum and bispectrum in redshift space
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微扰理论方法预测红移空间中星系功率谱和双谱的协方差矩阵
DOI：
10.1093/mnras/staa1940
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发表时间：
2019
影响因子：
4.8
通讯作者：
H. Seo
中科院分区：
文献类型：
--
作者：
Naonori S. Sugiyama;S. Saito;F. Beutler;H. Seo
本文利用微扰理论预测了功率谱和双谱的协方差矩阵，包括全非高斯贡献、红移空间失真、线性偏置效应和散粒噪声校正。为了量化红移空间扭曲效应，我们主要关注功率谱和双谱的单极和四极分量。我们首次通过计算5点和6点谱来预测功率谱和双谱之间的互协方差，以及红移空间中双谱的自协方差。我们通过将它们与多暗斑块模拟星表测量的协方差矩阵进行比较来测试我们计算的有效性，该星表旨在重现重子振荡光谱调查数据发布12版中测量的星系团。我们认为简单的前序微扰理论是可行的，因为片状模拟的散粒噪声修正比我们忽略的其他高阶项更重要。同时，我们确认了比较中的一些差异，特别是交叉协方差。我们讨论了这种差异的潜在来源。我们还表明，我们的PT模型很好地再现了功率谱和双谱的累积信噪比作为最大波数的函数，这意味着我们的PT模型成功地捕捉到了对协方差矩阵的重要贡献。
In this paper, we predict the covariance matrices of both the power spectrum and the bispectrum, including full non-Gaussian contributions, redshift space distortions, linear bias effects and shot-noise corrections, using perturbation theory (PT). To quantify the redshift-space distortion effect, we focus mainly on the monopole and quadrupole components of both the power and bispectra. We, for the first time, compute the 5- and 6-point spectra to predict the cross-covariance between the power and bispectra, and the auto-covariance of the bispectrum in redshift space. We test the validity of our calculations by comparing them with the covariance matrices measured from the MultiDark-Patchy mock catalogues that are designed to reproduce the galaxy clustering measured from the Baryon Oscillation Spectroscopic Survey Data Release 12. We argue that the simple, leading-order perturbation theory works because the shot-noise corrections for the Patchy mocks are more dominant than other higher-order terms we ignore. In the meantime, we confirm some discrepancies in the comparison, especially of the cross-covariance. We discuss potential sources of such discrepancies. We also show that our PT model reproduces well the cumulative signal-to-noise of the power spectrum and the bispectrum as a function of maximum wavenumber, implying that our PT model captures successfully essential contributions to the covariance matrices.
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星系双谱的偶极子
DOI：
10.1093/mnrasl/slz066
发表时间：
2019
期刊：
Letters
影响因子：
--
作者：
Clarkson C
通讯作者：
Clarkson C
影响因子：
6.5
作者：
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通讯作者：
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影响因子：
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作者：
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DESI 实验，Snowmass 2013 白皮书
DOI：
10.48550/arxiv.1308.0847
发表时间：
2013
期刊：
arXiv e-prints
影响因子：
--
作者：
Levi Michael
通讯作者：
Levi Michael